Date and Time of the Query: 2019-06-19 T12:56:14 PDT
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Notes for object NGC 4772

9 note(s) found in NED.

1. 2012ApJ...754...67F
Re:NGC 4772
NGC 4772 .SAS1..-The bulge morphology is smooth and featureless in HST F606W,
and the bulge is consequently classified as classical by Fisher & Drory (2008).
The [O III] map of Falcon-Barroso et al. (2006) shows almost counter-rotation
with respect to the stars in the central ~= +/- 5" (see also Haynes et al.
2000). Our data virtually only cover the bulge region. The velocity dispersion
profile is generally noisy with values between 100 km s^-1^ and 150 km s^-1^ but
features a clear central peak. The h_3_ moments are anti-correlated with
velocity and reach values of up to about +/- 0.07. h_4_ moments scatter around
values of 0.05 at all radii.

2. 2006MNRAS.369..529F
Re:NGC 4772
NGC 4772 is a galaxy located at the boundaries of the Virgo cluster (Haynes et
al. 2000). A strong dust lane is seen to the east. The stellar kinematics
display regular rotation along the major axis of the galaxy. The unsharp-masked
image reveals a small dusty disc in the centre of the galaxy, the orientation of
which seems consistent with that of the ionized gas in the central 5 arcsec. In
these regions, both the H{beta} and [O III] lines suggest ordered rotation for
the gas, almost in the opposite sense of the stars, in agreement with Haynes et
al. (2000). The ionized-gas emission also extends beyond the central regions, in
particular for the [O III] emission. The observed morphology is consistent with
the narrow-band observations of Haynes et al. (2000), suggesting that the gas
emission observed at the north-eastern and south-western corner of the SAURON
field comes from an outer ring of gas on the main galactic-disc plane. The [O
III] kinematics are more complex at larger radii, but suggest a warping of the
direction of maximum rotation towards the galaxy major axis.

3. 2002ApJS..143...73E
Re:NGC 4772
NGC 4772.---(R)SB0: Nuclear point source embedded in a bright,
circular bulge. Bulge is threaded by a long, broad, LSB bar. At the
ends of the bar, two very faint, narrow, smooth arms wrap around the
galaxy to form an outer ring.

4. 2001A&A...374..421B
Re:NGC 4772
4.7 NGC 4772
Haynes et al. (2000) considers NGC4772 as a case of apparent
counterrotation of the ionized gas versus the stars. The kinematical
decoupling of the nuclear ionized gas (r < 5" = 0.3 kpc), observed along
both the minor and the major axes, has been interpreted as the signature of
a misaligned embedded gas bar, rather than as evidence of counterrotation.
However, this Sa galaxy shares many features with other prototypical
counterrotators. Mimicking NGC 3626, the HI content of NGC 4772 is
distributed in two separate rings, probably non coplanar. As is the case
for NGC 3626, the central region of NGC 4772 is HI-poor. Furthermore, the
deep optical photometry of the galaxy reveals the presence of a round, low
surface brightness disk in the outer part, reminiscent of a similar feature
reported by Buta et al. (1995) in the Sab counterrotator NGC 7217.
The J = 1 - 0 spectrum of ^12^CO (Fig. 1) reveals the presence of
molecular gas (inside r = 1.5 kpc). The line profile, centered at
~1120 km s^-1^ and with FWHM ~ 300 km s^-1^, is slightly redshifted with
respect to the optically determined v_sys_ = 1040 km s^-1^ (the same as
derived from HI).
Emission in the J = 2 - 1 line is undetected, however. The molecular gas
mass within the central r = 1.5 kpc, derived from the ^12^CO(J = 1 - 0)
integrated intensity, would be M_mol_ = 5.4 x 10^7^ M_sun_.

5. 1999AJ....118.2331V
Re:NGC 4772
A pair of 80s F606W exposures of NGC 4772 is available. SN 1988E
was possibly a peculiar SN I (Pearce et al. 1990). Using the absolute SN
position from the Sternberg SN catalog, we find that the SN site is in a
region of faint, diffuse emission on the outskirts of this elliptical
galaxy, with no stellar objects within the 2" radius error circle.

6. 1997ApJS..112..391H
Re:NGC 4772
NGC 4772.--Broad H{alpha} is present unambiguously, as is evident from the wide
base on either side of the [N II] lines (Fig. 13h). Unfortunately, undulations
in the neighboring continuum compromise the accuracy of the fit to the broad
feature. Because of the steep velocity gradient in the inner rotation curve,
the narrow lines have a double-peaked or flat-topped profile, which was well
reproduced using two Gaussian components derived by fitting the [S II] lines.
Although the fit to [N II] {lambda}6583 shows considerable residuals, we chose
to impose stringent constraints because of the complexity of the blend.

7. 1995ApJS...98..477H
Re:NGC 4772
The [N II], H{alpha}, and [S II] lines have double-peaked profiles.
Inspection of the 2-D spectrum shows that the emission lines in the
nucleus are tilted with respect to the continuum, signifying a very steep
rotation curve.

8. 1973UGC...C...0000N
Re:UGC 08021
SA(s)a (de Vaucouleurs)

9. 1964RC1...C...0000d
Re:NGC 4772
Bright diffuse nucleus in a bulge. Smooth arcs or arms with a strong dark
lane on one side. Probably similar to NGC 4594. Classification is from a
weak plate.

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